We observed the flare stars AD Leonis , Wolf 424 , EQ Pegasi , EV Lacertae , and UV Ceti for nearly 135 hours .
These stars were observed between 63 and 83 MHz using the interferometry mode of the Long Wavelength Array .
Given that emission from flare stars is typically circularly polarized , we used the condition that any significant detection present in Stokes I must also be present in Stokes V at the same time in order for us to consider it a possible flare .
Following this , we made one marginal flare detection for the star EQ Pegasi .
This flare had a flux density of 5.91 Jy in Stokes I and 5.13 Jy in Stokes V , corresponding to a brightness temperature 1.75 \times 10 ^ { 16 } ( r / r _ { * } ) ^ { -2 } K .